Abstract
Abstract A very long and nearly straight H i filament at about −60 km s−1 in the southern Galactic hemisphere, seen nearly normal to the line of sight and well separated from low-velocity gas, has been studied in several ways in order to understand its physics, structure, and morphology. Gaussian analysis of 1800 profiles and examination of 140 declination–velocity cross sections shows that an underlying H i component, which is at least 15° long and about 1° wide, has a typical line width of 21 km s−1. It does not appear to be in thermal pressure equilibrium with its surroundings; rather, it may be confined by a magnetic field of 18 μG. Narrow, elongated features (threads), probably unresolved in the 4′ H i observations, have been identified within the boundaries of the filament. In general, each of these threads has two emission components, with line widths of the order of 8 and 3 km s−1, which may wind around each other. Analysis suggests that these cooler components have an average density of 29 cm−3 and may be confined by a magnetic field of 5 μG. These results, taken together, can be explained if this southern filament has magnetic substructure.
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